1. Mapping star formation at the peak epoch of galaxy formation and evolution “MAHALO-Subaru” MApping HAlpha and Lines of Oxygen with Subaru Taddy Kodama (Subaru Telescope), Yusei Koyama (Univ of Tokyo), Masao Hayashi (NAOJ), Kenichi Tadaki (NAOJ/UTokyo), Ichi Tanaka (Subaru Telescope), et al. Hα survey in CL0939 (z=0.41) (P19) [OII] survey in CL0218 (z=1.62) (P21) [OII] survey in CL0332 (z=1.61) (P20) A Subaru Intensive Program for S10B-S11A, started in last Sep.

2. z = 3 Nature? (intrinsic) earlier galaxy formation and evolution in high density regions Nurture? (external) galaxy-galaxy interaction/mergers, gas-stripping Spirals Lenticulars Ellipticals Star-forming (young) No/little SF (old) morphology ‐ density relation (Dressler 1980) z~0 log surface density (Mpc -2 ) Nature? (intrinsic) Need to go higher redshifts when it becomes more evident. Nurture? (external) Need to go outer infall regions to see directly what’s happening there. What’s the origin of the environmental dependence

3. ACS(3.5’) XMM 1.14 Panoramic Imaging and Spectroscopy of Cluster Evolution with Subaru Panoramic Imaging and Spectroscopy of Cluster Evolution with Subaru XMMJ2215.9-1738 22 15 58.5 -17 38 02.5 1.45 4.4 VRi’z’,NB CIGJ0218.3-0510 02 18 21.3 -05 10 27 1.62 BVRi’z’,NB z~1.5 XMM ~10 X-ray clusters (0.4 < z < 1.6) are completed Kodama et al. (2005) +update,NB ( )

4. 75% 50% 25% Cluster outskirts is the key environment for environmental effects Sharp color transition in the “medium-density” regions ( i.e. cluster outskirts / groups / filaments ) Kodama et al. (2001), see also Tanaka+05 and Koyama+08 ClusterGroup Field Log Σ (galaxy number density) (SFR Hα > 0.3M ☉ /yr) Hα (6563A)@z=0.4 NB921 z’ “Octopus cluster “ (CL0939 cluster at z=0.4)

5. BB selection (passive) + NB emitters (active) Hα emitters All true members phot-z member spec-z member Phot-z distribution of true members Kodama et al. (2004) CL0024 cluster (z=0.4) NB912 + Suprime-Cam Advantages of NB survey: (1)Good indicators of SFR, especially Hα (low reddening, well calibrated) (2)“Unbiased” sample (no pre-selection of targets is required). (3)“Complete” census of star forming galaxies to a certain limit in SFR. (4)Membership can be confirmed by the presence of emitters in NB +colours. (5)On top of the phot-z selected members (e.g. “passive” galaxies), we can pick out “active” galaxies which tend to be missed by phot-z selection.

6. Koyama et al. (2011), □ : Hα emitters □ : red Hα emitters □ : weak Hα emitters (SFR<0.75M ☉ /yr) (B-I>2) “Octopus cluster” (CL0939@z=0.41) see P19

7. Red Hα emitters in groups ! A significant fraction of red galaxies in groups show SF activities (dusty galaxies!) Koyama et al. (2011), N (all Hα emitters) N (red Hα emitters) see P19

8. J NB119 H  (6563A) @ z=0.81 ±2000km/s NB912 XCS J2215.9-1738 (z=1.46)RX J1716.6+6708 (z=0.81) MOIRCS + NB119 (Hα)Suprime-Cam + NB912 ([OII]) [OII] (3727A) of spec-z members Two examples of NB survey at z<1.5

9. Comparison of spatial distribution of star forming galaxies in cluster cores. Star forming activity in the core is much higher in the higher redshift cluster! Hα emitters at z=0.81 (RXJ1716)[OII] emitters at z=1.46 (XCS2215) Koyama, et al. (2010)Hayashi, et al. (2010) □□ ● phot-z members Lx=2.7×10 44 erg/sLx=4.4×10 44 erg/s 0.5 x R 200

10. z=0 z~0.8 z~1.5 : passive red galaxy : normal SF galaxy : dusty starburst ? Inside-Out Propagation of Star Formation Activity and its Truncation? Illustrated by Yusei Koyama Do we eventually see the reversal of the SFR-density relation at z>1.5 as a result of galaxy formation bias?

11. Narrow-band emitters (Hα, [OII]) surveys at 0.4 1.5) “MAHALO-Subaru” MApping HAlpha and Lines of Oxygen with Subaru clusters fields Subaru Intensive Program for S10B-S11A 10 nights allocation (6 nights completed under clear skies, 4 nights to come) (However, one of the MOIRCS chips was broken and FoV was halved in S10B…)

12. ClG J0218.3-0510 (z=1.62) in SXDFCL0332-2742 (z=1.61) in GOODS-S Two recently found, confirmed clusters at z~1.6 Kurk et al. (2009) (Papovich et al. 2010; Tanaka et al. 2010) X-ray detection (4.5σ) 9 spec-z members, σ=540km/s 42 spec-z members, σ=500km/s [OII] from z=1.61-1.62 Suprime-Cam

13. ClG J0218.3-0510 (z=1.62) in SXDF ● [OII] emitters (star-forming, AGN) ● Red sequence galaxies (~passive) Tadaki et al. in prep. see P21 a bright star cluster core ● ●

14. Star forming galaxies Red sequence galaxies ClG J0218.3-0510 (z=1.62) in SXDF Fraction of star forming Galaxies is higher in the cluster core !? Tadaki et al. in prep. Environmental variation see P21 “preliminary result”

15. [OII] emitters Ellipticals w/ GMASS spec-z Spirals w/ GMASS spec-z Irregulars w/ GMASS spec-z MUSIC obj. w/ 1.43<phot-z<1.77 GOODS-South CL0332-2742 (z=1.61) in GOODS-S Hayashi et al., in prep.see P20

16. Our unique NB-filter system on Subaru MOIRCS (+Suprime-Cam) specifically designed for this purpose! Brank field, multi-line NB survey at z=2.2 Secure redshifts of emitters Hβ/Hα (dust extinction) Lyα/Hα (escape fraction)

17. Tadaki et al., in preperation Hα emitters at z=2.2 traced by MOIRCS/NB209 Tadaki et al. (2011), in press GOODS-NSXDS 5 MOIRCS pointings 8 MOIRCS pointings NB209: ~2.5hrs Ks: UDS ~2-3×10 -17 erg/s/cm 2 ⇔ ~10-15 M ☉ /yr (3σ) “preliminary result”

18. “Mahalo-plot” (in analogy to “Madau-plot”) Emitters Only Tadaki et al. (2011), in press 〈 SSFR 〉 vs. z and environment for emitters Highly uncertain yet ! incompleteness cosmic variance …

19. Mapping gas and dust at the peak epoch of galaxy formation and evolution “MAHALO-ALMA” Molecular Associations with HAlpha and Lines of Oxygen probed with ALMA at ~100GHz (Band-3), highest sensitivity & largest FoV (1’) CO(2  1) for z=2  1, CO(3  2) for z=3  2 High density gas: Dust cotinuum: 850 μm – 1.1 mm, SFR~10M ☉ /yr at z>1.5 SFR~20M ☉ /yr (4hrs, 5σ) with CO(2-1)@z=1.5 and CO(3-2)@z=2.5 Internal kinematical structure: 0.01-0.1”(<1kpc) : gas in-/outflow, rotation

20. Mapping star formation at the peak epoch of galaxy formation and evolution “MAHALO-Subaru” MApping HAlpha and Lines of Oxygen with Subaru Taddy Kodama (Subaru Telescope), Yusei Koyama (Univ of Tokyo), Masao Hayashi (NAOJ), Kenichi Tadaki (NAOJ/UTokyo), Ichi Tanaka (Subaru Telescope), et al. Hα survey in CL0939 (z=0.41) (P19) [OII] survey in CL0218 (z=1.62) (P21) [OII] survey in CL0332 (z=1.61) (P20) A Subaru Intensive Program for S10B-S11A, started in last Sep.

22. Backup Slides

23. NB921/S-Cam [OII] @z=1.46 NB973/S-Cam [OII] @z=1.62 NB1657/MOIRCS Hα @z=1.52 1.46<z<1.65 is the golden redshift range for FMOS follow-up! [OII] + Hβ + [OIII] + Hα + [NII] Made by K. Tadaki  Dust extinction (Hα/Hβ), Metallicity (R23, N2), AGN ([OIII], [NII])

24. ClG J0218.3-0510 (z=1.62) in SXDF Tadaki et al., in prep. [OII] Hβ,[OIII]Hα NB973: ~10 hrs (Ota et al.) zR: 5.5hrs

25. Close-pair galaxies tend to have enhanced SF activities. Environmental dependenceStellar-mass dependence close-pair galaxies SFR SSFR SFR SSFR Hayashi et al., in prep. CL0332-2742 (z=1.61) in GOODS-S

26. Hα emitters survey in a proto-cluster 4C23.56 at z=2.483 with MOIRCS/NB2288 Tanaka, I., et al. (2011), in press Very strong star forming activities in the high-z proto-cluster!

27. Number density of QSOs Star formation density Bouwens et al. (2005) Galaxy/AGN evolution peaks at z~2 (T univ = 3.5 Gyrs) Fan et al. (2006)

28. Koyama et al. (2011) □ : Hα emitters □ : red Hα emitters □ : weak Hα emitters (SFR<0.75M ☉ /yr) (B-I>2)

29. NB973 emitters [OII] emitters at z=1.6 (Flux > 2.5 x 10 -17 erg/s/cm 2 ) >3 σ Hayashi et al., in prep. CL0332-2742 (z=1.61) in GOODS-S NB973: 7hrs zR: 3hrs

30. Tadaki et al. (2011), in press Hα emitters at z=2.2 in GOODS-N

31. Hα emitters at z=2.2 in SXDF 16 arcmin x 6 arcmnin Tadaki et al. In prep. NB209: ~2.5hrs Ks: UDS

32. Eastern Clump

33. A part of the FMOS-SSP -- to cover the highest-density regions --

34. Advantages of narrow-band surveys (Hα, [OII]) CL0939 cluster (z=0.4) (1)Good indicators of SFR, especially Hα (low reddening, well calibrated) (2)“Unbiased” sample (no pre-selection of targets is required). (3)Membership can be confirmed by the presence of emitters in NB +colours. (4)On top of the phot-z selected members (e.g. “passive” galaxies), we can pick out “active” galaxies which tend to be missed by phot-z selection. Blue galaxies tend to be missed by phot-z selection. Low-z tail is dominated by SF galaxies. Koyama+ (2011) □ Hα emitters